Extended AbstractThe Kwasan and Hida Observatories team (three of the authors but A. T.) observed the total solar eclipse of 11 July, 1991 with the multi-channel telescope at UABCS (Universidad Autonoma de Baja California Sur) campus in La Paz, Baja California Sur, Mexico. The primary purpose of our obsevation is to get high-resolution images of the inner corona at the wavelength of coronal emission lines and continuum shown in Table 1. Thanks to the clear sky and good seeing condition, we successfully got many images of high spatial resolution with photographic cameras and video recorders. Details of the observation have already been published by Kurokawaet al. (1992). In this paper, we present the results obtained from the photographic data reduction on fine structures of the inner corona. The procedure of photometrical measurement and image processing are fully described in another paper (Takeda, 1993).There have been published several observational works on the temperature structure of the coronal loops. Some authors proposed that hot coronal loops have cool cores (Foukal, 1975; Hanaokaet al., 1988), but others denied such coaxial models (Chenget al., 1980; Dere, 1982). Our high-resolution images obtained at the eclipse enables us to compare the positions of the loops seen in different emission lines of different ionization temperatures more precisely than any other previous observations. Main results are summarized as follows.